{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:EFNHOY7Y42B2RJ23SXWGJMW76C","short_pith_number":"pith:EFNHOY7Y","schema_version":"1.0","canonical_sha256":"215a7763f8e683a8a75b95ec64b2dff0a9584c045c779afbf96433d0bde6da5a","source":{"kind":"arxiv","id":"0901.2930","version":2},"attestation_state":"computed","paper":{"title":"The Kiloparsec-Scale Kinematics of High-Redshift Star-Forming Galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Alice E. Shapley, Charles C. Steidel, David R. Law, Dawn K. Erb, James E. Larkin, Max Pettini, Shelley A. Wright","submitted_at":"2009-01-19T21:00:27Z","abstract_excerpt":"We present the results of a spectroscopic survey of the kinematic structure of star-forming galaxies at redshift z ~ 2 - 3 using Keck/OSIRIS integral field spectroscopy. Our sample is comprised of 12 galaxies between redshifts z ~ 2.0 and 2.5 and one galaxy at z ~ 3.3 which are well detected in either HAlpha or [O III] emission. These observations were obtained in conjunction with the Keck laser guide star adaptive optics system, with a typical angular resolution after spatial smoothing ~ 0.15\" (approximately 1 kpc at the redshift of the target sample). At most five of these 13 galaxies have s"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"0901.2930","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2009-01-19T21:00:27Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"9ebcd4d585f0b2e1a37305034e9bae93ce58f41426b0348f8ebc4ccc5849c1ee","abstract_canon_sha256":"e48ac7ba3c1b976040ed20c21ab7058c0b179dd3f50086385d46895a4b011d37"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:35:06.403772Z","signature_b64":"ezGG9Y/mjvJWd3roxy9oE013r0LPwHyW89RRowOqiIvdWpUer5cvlnHdoz+d3JLQtgodejZqLonSP6Le81/0Ag==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"215a7763f8e683a8a75b95ec64b2dff0a9584c045c779afbf96433d0bde6da5a","last_reissued_at":"2026-05-18T02:35:06.403240Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:35:06.403240Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Kiloparsec-Scale Kinematics of High-Redshift Star-Forming Galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Alice E. Shapley, Charles C. Steidel, David R. Law, Dawn K. Erb, James E. Larkin, Max Pettini, Shelley A. Wright","submitted_at":"2009-01-19T21:00:27Z","abstract_excerpt":"We present the results of a spectroscopic survey of the kinematic structure of star-forming galaxies at redshift z ~ 2 - 3 using Keck/OSIRIS integral field spectroscopy. Our sample is comprised of 12 galaxies between redshifts z ~ 2.0 and 2.5 and one galaxy at z ~ 3.3 which are well detected in either HAlpha or [O III] emission. These observations were obtained in conjunction with the Keck laser guide star adaptive optics system, with a typical angular resolution after spatial smoothing ~ 0.15\" (approximately 1 kpc at the redshift of the target sample). At most five of these 13 galaxies have s"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0901.2930","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"0901.2930","created_at":"2026-05-18T02:35:06.403331+00:00"},{"alias_kind":"arxiv_version","alias_value":"0901.2930v2","created_at":"2026-05-18T02:35:06.403331+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0901.2930","created_at":"2026-05-18T02:35:06.403331+00:00"},{"alias_kind":"pith_short_12","alias_value":"EFNHOY7Y42B2","created_at":"2026-05-18T12:25:59.703012+00:00"},{"alias_kind":"pith_short_16","alias_value":"EFNHOY7Y42B2RJ23","created_at":"2026-05-18T12:25:59.703012+00:00"},{"alias_kind":"pith_short_8","alias_value":"EFNHOY7Y","created_at":"2026-05-18T12:25:59.703012+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2606.23456","citing_title":"Stellar winds of O-type stars traced by high ionization fine-structure emission lines with JWST/MIRI","ref_index":5,"is_internal_anchor":true},{"citing_arxiv_id":"2606.25164","citing_title":"Dust destruction signals shock-accelerated outflows in the nearby active galaxy NGC 1068","ref_index":274,"is_internal_anchor":true},{"citing_arxiv_id":"2606.25164","citing_title":"Dust destruction signals shock-accelerated outflows in the nearby active galaxy NGC 1068","ref_index":274,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EFNHOY7Y42B2RJ23SXWGJMW76C","json":"https://pith.science/pith/EFNHOY7Y42B2RJ23SXWGJMW76C.json","graph_json":"https://pith.science/api/pith-number/EFNHOY7Y42B2RJ23SXWGJMW76C/graph.json","events_json":"https://pith.science/api/pith-number/EFNHOY7Y42B2RJ23SXWGJMW76C/events.json","paper":"https://pith.science/paper/EFNHOY7Y"},"agent_actions":{"view_html":"https://pith.science/pith/EFNHOY7Y42B2RJ23SXWGJMW76C","download_json":"https://pith.science/pith/EFNHOY7Y42B2RJ23SXWGJMW76C.json","view_paper":"https://pith.science/paper/EFNHOY7Y","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0901.2930&json=true","fetch_graph":"https://pith.science/api/pith-number/EFNHOY7Y42B2RJ23SXWGJMW76C/graph.json","fetch_events":"https://pith.science/api/pith-number/EFNHOY7Y42B2RJ23SXWGJMW76C/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EFNHOY7Y42B2RJ23SXWGJMW76C/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EFNHOY7Y42B2RJ23SXWGJMW76C/action/storage_attestation","attest_author":"https://pith.science/pith/EFNHOY7Y42B2RJ23SXWGJMW76C/action/author_attestation","sign_citation":"https://pith.science/pith/EFNHOY7Y42B2RJ23SXWGJMW76C/action/citation_signature","submit_replication":"https://pith.science/pith/EFNHOY7Y42B2RJ23SXWGJMW76C/action/replication_record"}},"created_at":"2026-05-18T02:35:06.403331+00:00","updated_at":"2026-05-18T02:35:06.403331+00:00"}